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J. P. Leahy and P. Parma, in Extragalactic Radio Sources. From Beams to Jets , edited by J. Roland, H. Sol, and G. Pelletier (1992) pp. 307–308
1992
Earlier work this paper cites.
M. Campanelli and C. O. Lousto, Phys. Rev. D59
1999
Earlier work this paper cites.
O. Dreyer, B. Krishnan, D. Shoemaker, and E. Schnetter, Phys. Rev. D67
2003
Earlier work this paper cites.
M. Ansorg, B. Brügmann, and W. Tichy, Phys. Rev. D70
2004
Earlier work this paper cites.
E. Schnetter, S. H. Hawley, and I. Hawke, Class. Quant. Grav. 21
2004
Earlier work this paper cites.
J. Thornburg, Class. Quant. Grav. 21
2004
Earlier work this paper cites.
F. Pretorius, Phys. Rev. Lett. 95
2005
Earlier work this paper cites.
Y. Zlochower, J. G. Baker, M. Campanelli, and C. O. Lousto, Phys. Rev. D72
2005
Earlier work this paper cites.
J. G. Baker, J. Centrella, D.-I. Choi, M. Koppitz, and J. van Meter, Phys. Rev. Lett. 96
2006
Earlier work this paper cites.
A. Buonanno, Y. Chen, and T. Damour, Phys. Rev. D74
2006
Earlier work this paper cites.

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2014

Lousto, Carlos O., Healy, James

We study binary spinning black holes to display the long term individual spin dynamics.

We perform a full numerical simulation starting at an initial proper separation of $d\approx25M$ between equal mass holes and evolve them down to merger for nearly 48 orbits, 3 precession cycles, and half of a flip-flop cycle.
The simulation lasts for $t=20000M$ and displays a total change in the orientation of the spin of one of the black holes from initially aligned with the orbital angular momentum to a complete anti-alignment after half of a flip-flop cycle.
We compare this evolution with an integration of the 3.5 Post-Newtonian equations of motion and spin evolution to show that this process continuously flip-flops the spin during the lifetime of the binary until merger.

J. P. Leahy and P. Parma, in Extragalactic Radio Sources. From Beams to Jets , edited by J. Roland, H. Sol, and G. Pelletier (1992) pp. 307–308
1992
Earlier work this paper cites.
M. Campanelli and C. O. Lousto, Phys. Rev. D59
1999
Earlier work this paper cites.
O. Dreyer, B. Krishnan, D. Shoemaker, and E. Schnetter, Phys. Rev. D67
2003
Earlier work this paper cites.
M. Ansorg, B. Brügmann, and W. Tichy, Phys. Rev. D70
2004
Earlier work this paper cites.
E. Schnetter, S. H. Hawley, and I. Hawke, Class. Quant. Grav. 21
2004
Earlier work this paper cites.
J. Thornburg, Class. Quant. Grav. 21
2004
Earlier work this paper cites.
F. Pretorius, Phys. Rev. Lett. 95
2005
Earlier work this paper cites.
Y. Zlochower, J. G. Baker, M. Campanelli, and C. O. Lousto, Phys. Rev. D72
2005
Earlier work this paper cites.
J. G. Baker, J. Centrella, D.-I. Choi, M. Koppitz, and J. van Meter, Phys. Rev. Lett. 96
2006
Earlier work this paper cites.
A. Buonanno, Y. Chen, and T. Damour, Phys. Rev. D74
2006
Earlier work this paper cites.